Large scale flows in the solar convection zone

We discuss the current theoretical understanding of the large scale flows observed in the solar convection zone, namely the differential rotation and meridional circulation. Based on multi-D numerical simulations we describe which physical processes are at the origin of these large scale flows, how they are maintained and what sets their unique profiles. We also discuss how dynamo generated magnetic field may influence such a delicate dynamical balance and lead to a temporal modulation of the amplitude and profiles of the solar large scale flows.

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An edited version of this paper was published by Springer. Copyright Springer Science+Business Media B.V. 2008.


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Author Brun, Allan
Rempel, Matthias
Publisher UCAR/NCAR - Library
Publication Date 2009-04-01T00:00:00
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Topic Category geoscientificInformation
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Metadata Date 2023-08-18T18:57:24.724493
Metadata Record Identifier edu.ucar.opensky::articles:15393
Metadata Language eng; USA
Suggested Citation Brun, Allan, Rempel, Matthias. (2009). Large scale flows in the solar convection zone. UCAR/NCAR - Library. http://n2t.net/ark:/85065/d7ms3ts1. Accessed 20 July 2025.

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